{
  "submitter": "Valentina Panteleeva at Ioffe Institute <panteleevav228@gmail.com>",
  "eventType": [
    "GRB",
    "Gamma-ray Transient"
  ],
  "eventId": "GRB 261029A",
  "body": "V. Panteleeva, D. Frederiks, A. Lysenko, A. Ridnaia, D. Svinkin,\nA. Tsvetkova,  M. Ulanov, and T. Cline,\non behalf of the Konus-Wind team, report:\n\nThe long-duration GRB 261029A\n(Fermi-GBM detection: The Fermi GBM team, GCN 46071;\nScotton, GCN 46098;\nSVOM-ECLAIRs detection: Goto et al., GCN 46072;\nFermi-LAT detection: Longo et al., GCN 46085;\nAstroSat CZTI detection: Salunke et al., GCN 46089;\nCALET detection: Marrocchesi et al., GCN 46095;\nSVOM-GRM observation: Yu et al., GCN 46096;\nNuSTAR detection: Waratkar & Grefenstette, GCN 46100;\nGECAM-B detection: Yu & Xiong, GCN 46108;\nGlowbug detection: Cheung et al., GCN 46112)\ntriggered Konus-Wind at T0=05228.129 s UT (01:27:08.129).\n\nThe burst light curve shows a multipeaked structure\nwhich starts at ~T0-0.4 s and has a total duration of ~112 s.\nThe emission is seen up to ~60 MeV.\n\nThe Konus-Wind light curve of this GRB is available at\nhttp://www.ioffe.ru/LEA/GRBs/GRB261029_T05228/\n\nAs observed by Konus-Wind, the burst\nhad the total fluence of 1.97(-0.11,+0.11)x10^-4 erg/cm2,\nand the 64-ms peak flux, measured from T0+38.848 s,\nof 2.03(-0.19,+0.19)x10^-5 erg/cm2/s\n(both in the 20 keV - 10 MeV energy range).\n\nThe time-averaged spectrum of the burst\n(measured from T0 to T0+112.640 s)\nis best fit in the 20 keV - 10 MeV range\nby the GRB (Band) model with the following parameters:\nthe low-energy photon index alpha = -0.82(-0.05,+0.05),\nthe high energy photon index beta = -2.13(-0.10,+0.08),\nthe peak energy Ep = 590(-44,+47) keV\n(chi2 = 83/97 dof).\n\nThe spectrum near the maximum count rate\n(measured from T0+37.120 to T0+38.912 s)\nis best fit in the 20 keV - 10 MeV range\nby the GRB (Band) model with the following parameters:\nthe low-energy photon index alpha = -0.66(-0.05,+0.06),\nthe high energy photon index beta = -2.58(-0.27,+0.18),\nthe peak energy Ep = 753(-64,+68) keV\n(chi2 = 61/66 dof).\n\nAssuming the redshift z=3.270 (Cotter et al., GCN 46081)\nand a standard cosmology with H_0 = 67.3 km/s/Mpc, Omega_M = 0.315,\nand Omega_Lambda = 0.685 (Planck Collaboration, 2014),\nwe estimate the following rest-frame parameters:\nthe isotropic energy release E_iso is  4.56(-0.25,+0.25)x10^54 erg,\nthe peak luminosity L_iso is 2.03(-0.19,+0.19)x10^54 erg/s,\nthe rest-frame peak energy of the time-averaged spectrum\nEp,i,z is 2518(-188,+199) keV and the spectrum near the maximum count rate\nEp,p,z is 3217(-272,+291) keV.\n\nWith the obtained estimates, GRB 261029A is inside 68% prediction bands for\nboth the 'Amati' and the 'Yonetoku' relations derived for the sample of >300 long\nKW GRBs with known redshifts (Tsvetkova et al., 2017; Tsvetkova et al., 2021),\nsee http://www.ioffe.ru/LEA/GRBs/GRB261029_T05228/GRB261029A_rest_frame.pdf\n\nAll the quoted errors are at the 68% confidence level.\nAll the quoted values are preliminary.",
  "circularId": 46136,
  "subject": "Konus-Wind detection of GRB 261029A",
  "submittedHow": "web",
  "createdOn": 1793703189812,
  "format": "text/plain"
}